带电Kalb-Ramond黑洞中薄盘与厚盘的吸积动力学
Accretion dynamics of thin and thick disks in charged Kalb-Ramond black holes
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中文总结 AI 辅助
研究带电Kalb-Ramond黑洞的薄、厚吸积盘动力学，约束其参数空间，揭示电荷与洛伦兹对称性破缺对吸积流观测特性的联合影响，为KR引力提供潜在强引力信号。
中文摘要 AI 辅助
本工作研究Kalb-Ramond（KR）引力中带电、静态、球对称黑洞的吸积特性，其中无量纲参数$l$表征自发洛伦兹对称性破缺。我们首先通过将该类解的预测阴影半径与事件视界望远镜对人马座A*观测推断的界限进行比较，约束自由电荷与KR参数空间$(Q,l)$。电荷的引入造成$Q$与$l$之间的简并，扩大了与观测阴影尺寸相容的区域，得到宽泛约束$-0.3900 \leq l \leq 0.1898$，且部分相容参数空间延伸至裸奇点区域。随后，我们在上述约束下研究带电KR黑洞周围的相对论吸积盘：对于几何薄盘，计算时间平均能流、温度分布、发射光谱、时间平均扭矩及质能辐射转换效率，发现$l$值越高辐射输出越大，$l$值越低则抑制辐射输出，且与电荷耦合时该效应被放大；对于几何厚、角动量恒定的 torus 形盘，洛伦兹对称性破缺会移动特征轨道半径、压缩平衡构型的径向范围、缩小支撑有限平衡 torus 的区间，并将稳态流体拓扑移至该区间外的开放无约束构型。这些结果表明电荷与自发洛伦兹对称性破缺如何共同影响观测约束及黑洞吸积流的结构与发射特性，为强引力 regime 中KR引力提供潜在信号。
英文摘要
In this work, we investigate the accretion properties of an electrically charged, static, spherically symmetric black hole in Kalb-Ramond (KR) gravity, where a dimensionless parameter $l$ characterizes spontaneous Lorentz symmetry-breaking. We first constrain the free charge and KR parameter space, $(Q,l)$, by comparing the predicted shadow radius of this family of solutions with the bounds inferred from Event Horizon Telescope observations of Sagittarius A*. The inclusion of electric charge introduces a degeneracy between $Q$ and $l$, enlarging the region compatible with the observed shadow size and yielding the broad constraint $-0.3900 \leq l \leq 0.1898$, with part of the compatible parameter space extending into the naked-singularity sector. We then investigate relativistic accretion disks around the charged KR black hole within the above constraints. For geometrically thin disks, we compute the time averaged energy flux, temperature distribution, emission spectrum, time averaged torque, and mass-to-radiation conversion efficiency, finding that the radiative output increases for higher values of $l$, while lower values of $l$ suppress it. Furthermore, when coupled with the electric charge this effect is amplified. For geometrically thick, constant-angular momentum tori-shaped disks, Lorentz symmetry-breaking shifts the characteristic orbital radii, compresses the radial extent of equilibrium configurations, narrows the interval supporting finite equilibrium tori, and shifts the stationary-fluid topology toward open and unconfined configurations outside that interval. These results show how charge and spontaneous Lorentz symmetry-breaking jointly affect observational constraints and the structure and emission properties of black hole accretion flows, providing potential signatures of KR gravity in the strong-gravity regime.
发表机构
- Faculdade de Física, Universidade Federal do Pará（帕拉联邦大学物理学院）
- Programa de Pós-Graduação em Física, Universidade Federal do Sul e Sudeste do Pará（帕拉南部和东南部联邦大学物理研究生项目）
- Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências da Universidade de Lisboa（里斯本大学科学学院天体物理学与空间科学研究所）
- Departamento de Física, Faculdade de Ciências da Universidade de Lisboa（里斯本大学科学学院物理系）
- Faculdade de Ciências Exatas e Tecnologia, Universidade Federal do Pará（帕拉联邦大学精确科学与技术学院）
- Universidad Complutense de Madrid（马德里康普顿斯大学）
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